<i>Euclid</i> preparation

This paper describes the objectives, design, and findings of the pre-launch ground characterisation campaigns of the Euclid infrared detectors. The aim of the ground characterisations is to evaluate the performance of the detectors, to calibrate the pixel response, and to derive the pixel response correction methods. The detectors have been tested and characterised in the facilities set up for this purpose. The pixel properties, including baseline, bad pixels, quantum efficiency, inter pixel capacitance, quantum efficiency, dark current, readout noise, conversion gain, response non-linearity, and image persistence were measured and characterised for each pixel. We describe in detail the test flow definition that allows us to derive the pixel properties and we present the data acquisition and data quality check software implemented for this purpose. We also outline the measurement protocols of all the pixel properties presented and we provide a comprehensive overview of the performance of the Euclid infrared detectors as derived after tuning the operating parameters of the detectors. The main conclusion of this work is that the performance of the infrared detectors Euclid meets the requirements. Pixels classified as non-functioning accounted for less than 0.2% of all science pixels. The interpixel capacitance (IPC) coupling is minimal, the cross-talk between adjacent pixels is less than 1% between adjacent pixels, and 95% of the pixels show a quantum efficienty (QE) greater than 80% across the entire spectral range of the Euclid mission. The conversion gain is approximately 0.52 ADU/e − , with a variation of less than 1% between channels of the same detector. The reset noise is approximately equal to 23 ADU rms after reference pixel correction. The readout noise of a single frame is approximately 13 e − rms while the signal estimator noise is measured at 7 e − rms in photometric mode and 9 e − rms in spectroscopic acquisition mode. The deviation from linear response at signal levels up to 80 ke − is less than 5% for 95% of the pixels. Median persistence amplitudes are less than 0.3% of the signal, though persistence exhibits significant spatial variation and differences between detectors.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2025-11-14
DOI
https://doi.org/10.1051/0004-6361/202555777
Primary Topic
Advanced Semiconductor Detectors and Materials
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article
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Euclid preparation

M Viel, R. Laureijs, G. Seidel, A. Ealet et al.
Astronomy and Astrophysics
Advanced Semiconductor Detectors and Materials
article

Euclid preparation

M Viel, R. Laureijs, G. Seidel, A. Ealet, F Passalacqua, J. Hjorth, Will J. Percival, F Raison, M. Ballardini, P. Tallada-Crespí, S Sacquegna, A. Pisani, F. Gianotti, M. Schirmer, D. Le Mignant, C. Sirignano, E. Gaztanaga, S Toft, I. Hook, M. Kunz, M. Trifoglio, G. Sirri, F. Dubath, J Brinchmann, W.G Hartley, R. Kohley, J. Carretero, D. B. Sanders, F. Marulli, J. García-Bellido, A.G Ferrari, A. Navarro-Alsina, C. Giocoli, M. Tenti, L Patrizii, R. Barbier, Paola Dimauro, F. Torradeflot, A. Kiessling, A. Troja, F Caro, J.R. Weaver, M. Jhabvala, A. Díaz‐Sánchez, J.-L Gimenez, G. Gozaliasl, E. Sellentin, M. Tewes, Harald J. Hoekstra, S. Mei, S. Bardelli, G. Desprez, P. Reimberg, E. Borsato, F Faustini, E Medinaceli, Francisco Javier Castander, Daniele Bertacca, C. Padilla, P.W. Morris, M. Magliocchetti, G Castignani, S. Nadathur, A.R. Cooray, L. Moscardini, C. Baccigalupi, S.-M Niemi, T. Schrabback, L. Gabarra, M Miluzio, C. J. A. P. Martins, J Le Graet, Giovanni Riccio, S. Andreon, S. V. H. Haugan, D. Vergani, R. Massey, A Enia, E. Romelli, S. Andreon, G. Leroy, Valérie Gautard, R. Toledo-Moreo, P. Schneider, B. Camacho Quevedo, S Bruton, M. Moresco, K Pedersen, R. Saglia, B. R. Granett, D. Sapone, T. Castro, M. Meneghetti, H. J. McCracken, N. Martinet, G. Testera, L. Patrizii, C. Colodro-Conde, A. Veropalumbo, T.I Liaudat, Franck Ducret, K. Ganga, Simon Conseil, M. Martinelli, C. Mancini, L. Caillat, C. Burigana, A. M. Di Giorgio, S Quai, Christopher J. Conselice, A. Biviano, I. Tutusaus, S. Davini, Julien Lesgourgues, I Risso, K Paterson, V. Allevato, A. Bonchi, E. Zucca, Fabio Lepori, P. Hudelot, L. Conversi, S. Escoffier, K. George, L Blot, E. Maiorano, A. Tsyganov, S Serrano, Maria Lembo, B. Gillis, M. Castellano, S. Ventura, M Sahlén, V. Scottez, F. De Paolis, S Casas, E. Merlin, R. B. Metcalf, J. Rhodes, D. Potter, R. Chary, Sandor Kruk, C. Tao, M. Pöntinen, M. Giulietti, S. Marcin, F. M. Zerbi, M. Béthermin, E. Branchini, A. Balestra, K. Jahnkę, A. M. N. Ferguson, B. Altieri, M. Farina, R. Laureijs, Antonello Calabrò, J. C. Salvignol, A. Venhola, L. Guzzo, E. Sefusatti, C.A.J Duncan, S Anselmi, J. Weller, H Kurki-Suonio, S. Ligori, M Fumana, R. Farinelli, F. Giacomini, Augustyn Waczynski, M. Melchior, E Prieto, E. Franceschi, A. Fontana, J.A Schewtschenko, A. Cimatti, ENRIQUE GAZTAÑAGA, J Martín-Fleitas, Yang Wang, W. Gillard, M. Brescia, M. Scodeggio, Q. Le Boulc'h, S. Dusini, M. Radovich, Pardis Simon, Cherry A. Murray, H. Cho, C. Giocoli, Y. Mellier, J. Gracia-Carpio, I.T Andika, R. Cabanac, S. Ferriol, A. Finoguenov, A Secroun, Z. Sakr, G. Polenta, F. Hormuth, K Tanidis, L. Legrand, K. Kiiveri, E. Bozzo, Romain Teyssier, LAURENCE C. SMITH, A. Blanchard, V. Pettorino, G.F Lesci, K. C. Chambers, F. Finelli⋆, A. Costille, T Gasparetto, R. Rébolo, P.-F Rocci, O. Mansutti, A da Silva, E. Keihänen, M Roncarelli, Yann Philippe Charles, Richard Foltz, M. Carle, R. Nakajima, S. Cavuoti, Krishna Naidoo, N. Auricchio, H. Degaudenzi, S Galeotta, S Camera, A. Cappi, S. Kermiche, H.I Teplitz, E Sarpa, Stefanie Wachter, G. Congedo, J. M. Diego, A. A. Franco, P. B. Lilje, Chiara Moretti, D. Tavagnacco, A.N. Taylor, C.S. Carvalho, L.A. Popa, S. Paltani, M. Sereno, R. da Silva, M. Poncet, A.M.C Le Brun, Vinay Kansal, M. Douspis, T. Maciaszek, C. Porciani, G. Mainetti, O. Marggraf, Y. Akrami, G. De Lucia, F. Atrio‐Barandela, H. M. Courtois, R. C. Nichol, Laurent Martin, F. Cogato, D Sciotti, P Casenove, S. Tosi, A. Da Silva, A. J. Hall, L. Maurin, Yuan Fang, C. M. Gutiérrez, J.E. Kajava, Y. W. Kang, M. Baldi, M Bolzonella, N. Aghanim, B. Sartoris, G. Meylan, S. Paltani, E. Rossetti, W. Holmes, C Neissner, D. Maino, J. Valiviita, X. Dupac, N Mauri, M. Archidiacono, C.C Kirkpatrick, I. Tereno, A. Zacchei, P Battaglia, J. Macias-Perez, L. Valenziano, O Cucciati, G. Zamorani, M. Wiesmann, R. Kohley, W. A. Holmes, P. Liebing, X. Dupac, G. Maggio, L Stanco, S. Maurogordato, S. Pires, J.A. Escartin Vigo, J. Zoubian, B. Kubik, D. Di Ferdinando, H. Hildebrandt, M. Tucci, I. Lloro, P Monaco, Y. Ascasíbar, M. Seiffert, S. Fotopoulou, S Mei, N. Fourmanoit, G Setnikar, A Mora, Anne Bonnefoi, G Verza, G. Smadja, M.L Brown, J. C. Clemens, M. N. Bremer, C Valieri, M Guidi, M. Kümmel, G. Morgante, Francis Bernardeau, C. Bonoli, A. Renzi, A. Derosa, A Montoro, L. Leuzzi
article en

Abstract

This paper describes the objectives, design, and findings of the pre-launch ground characterisation campaigns of the Euclid infrared detectors. The aim of the ground characterisations is to evaluate the performance of the detectors, to calibrate the pixel response, and to derive the pixel response correction methods. The detectors have been tested and characterised in the facilities set up for this purpose. The pixel properties, including baseline, bad pixels, quantum efficiency, inter pixel capacitance, quantum efficiency, dark current, readout noise, conversion gain, response non-linearity, and image persistence were measured and characterised for each pixel. We describe in detail the test flow definition that allows us to derive the pixel properties and we present the data acquisition and data quality check software implemented for this purpose. We also outline the measurement protocols of all the pixel properties presented and we provide a comprehensive overview of the performance of the Euclid infrared detectors as derived after tuning the operating parameters of the detectors. The main conclusion of this work is that the performance of the infrared detectors Euclid meets the requirements. Pixels classified as non-functioning accounted for less than 0.2% of all science pixels. The interpixel capacitance (IPC) coupling is minimal, the cross-talk between adjacent pixels is less than 1% between adjacent pixels, and 95% of the pixels show a quantum efficienty (QE) greater than 80% across the entire spectral range of the Euclid mission. The conversion gain is approximately 0.52 ADU/e − , with a variation of less than 1% between channels of the same detector. The reset noise is approximately equal to 23 ADU rms after reference pixel correction. The readout noise of a single frame is approximately 13 e − rms while the signal estimator noise is measured at 7 e − rms in photometric mode and 9 e − rms in spectroscopic acquisition mode. The deviation from linear response at signal levels up to 80 ke − is less than 5% for 95% of the pixels. Median persistence amplitudes are less than 0.3% of the signal, though persistence exhibits significant spatial variation and differences between detectors.

Astronomy and AstrophysicsVol. 707
Université Claude Bernard Lyon 1 (FR), University of Geneva (CH), Institució Catalana de Recerca i Estudis Avançats (ES), Leiden University (NL), California Institute of Technology (US), University of Copenhagen (DK), Centre National de la Recherche Scientifique (FR), Goddard Space Flight Center (US), University of Hawaii System (US), Jet Propulsion Laboratory (US), Universidade Federal de Ciências da Saúde de Porto Alegre (BR), Université Toulouse III - Paul Sabatier (FR), Consejo Superior de Investigaciones Científicas (ES), University of Bonn (DE), Scuola Internazionale Superiore di Studi Avanzati (IT), University of Padua (IT), University of Lisbon (PT), University of Salento (IT), University of Waterloo (CA), Universidad de La Laguna (ES), Stockholm University (SE), University of Groningen (NL), Université Fédérale de Toulouse Midi-Pyrénées (FR), Lyon College (US), Université Catholique de Lille (FR), Perimeter Institute (CA), University of Oslo (NO), Universidad de Salamanca (ES), Institute for High Energy Physics (ES), University of Milan (IT), Durham University (GB), Universität Innsbruck (AT), University of Saint Joseph (US), Princeton University (US), University of Ferrara (IT), Université Côte d'Azur (FR), University of Zurich (CH), University of California, Irvine (US), Université Paris Cité (FR), Aix-Marseille Université (FR), Heidelberg University (DE), University of Cambridge (GB), Commissariat à l'Énergie Atomique et aux Énergies Alternatives (FR), Université Paris Sciences et Lettres (FR), Université Paris-Saclay (FR), Centre National d'Études Spatiales (FR), Arcetri Astrophysical Observatory (IT), Helsinki Institute of Physics (FI), Astronomical Observatory of Rome (IT), Agenzia Spaziale Italiana (IT), Trieste Astronomical Observatory (IT), Institut d'Astrophysique de Paris (FR), Astronomical Observatory of Capodimonte (IT), European Space Agency (FR), Laboratoire AstroParticule et Cosmologie (FR), Observatoire astronomique de Strasbourg (FR), Brera Astronomical Observatory (IT), University of California System (US), University of Surrey (GB), FHNW University of Applied Sciences and Arts Northwestern Switzerland (CH), Universidad Politécnica de Cartagena (ES), Department of Space (IN), University of Bristol (GB), Sorbonne Université (FR), University of Oxford (GB), Park University (US), Osservatorio astronomico di Bologna (IT), Astrophysique, Instrumentation et Modélisation (FR), Valongo Observatory (BR), Institute of Astrophysics and Space Sciences (PT), ARC Centre of Excellence for Dark Matter Particle Physics (AU), Sorbonne Paris Cité (FR), Max Planck Institute for Extraterrestrial Physics (DE), Institut d'Estudis Espacials de Catalunya (ES), European Space Astronomy Centre (ES), Istituto Nazionale di Fisica Nucleare, Sezione di Lecce (IT), Istituto Nazionale di Fisica Nucleare, Sezione di Torino (IT), Institute for Space Astrophysics and Planetology (IT), Institut d'Astrophysique Spatiale (FR), Max Planck Institute for Astrophysics (DE), International University of Beirut (LB), Institut Català de Ciències del Clima (ES), Istituto Nazionale di Fisica Nucleare, Sezione di Padova (IT), Osservatorio Astrofisico di Torino (IT), Royal Observatory (GB), Istituto Nazionale di Fisica Nucleare, Sezione di Ferrara (IT), SKA Observatory (GB), Istituto Nazionale di Fisica Nucleare, Sezione di Napoli (IT), Centro de Astrofísica da Universidade do Porto (PT), Max Planck Institute for Astronomy (DE), Institute of Space Sciences (ES), Laboratoire de Physique Théorique (FR), DAWN Center for Independent Living (US), Centre for Theoretical Physics and Astrophysics (UZ), Istituto di Radioastronomia di Bologna (IT), Kavli Institute for the Physics and Mathematics of the Universe (JP), Federico II University Hospital (IT), Unidades Centrales Científico-Técnicas (ES), Mathematical Institute of the Slovak Academy of Sciences (SK), Institute of Astronomy (RU), Carnegie Observatories (US), Institute of Theoretical Physics (CN), Istituto Nazionale di Fisica Nucleare, Sezione di Genova (IT), Observatoire de la Côte d’Azur (FR), CEA Paris-Saclay (FR), Naples Anesthesia & Physician Associates (US), Instituto de Astrofísica de Canarias (ES), Felix Scholarship (GB), Astronomical Institute of the Slovak Academy of Sciences (SK), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (IT), Institute of Space Science - INFLPR Subsidiary (RO), Computing Center (RU), Centre de Calcul de l’Institut National de Physique Nucléaire et de Physique des Particules (FR), Astronomy and Space (AU), Istituto Nazionale di Fisica Nucleare, Sezione di Bologna (IT), Port d'Informació Científica (ES), Istituto Nazionale di Fisica Nucleare, Sezione di Trieste (IT), Institute for Fundamental Physics of the Universe (IT), Instituto de Física de Cantabria (ES), Flatiron Health (United States) (US), St. Joseph Medical Center (US), Istituto Nazionale di Fisica Nucleare, Sezione di Roma I (IT), Osservatorio Astronomico di Padova (IT), Bristol Robotics Laboratory (GB), Institut de Physique Théorique (FR), European Space Research Institute (IT), Institut de Recherche sur les Lois Fondamentales de l'Univers (FR), Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (ES), Institut de Recherche en Astrophysique et Planétologie (FR), Infrared Processing and Analysis Center (US), Osservatorio di Astrofisica e Scienza dello Spazio, Flatiron Institute (US), European Space Research and Technology Centre (NL), University College London (GB), Imperial College London (GB), UK Astronomy Technology Centre (GB), École Polytechnique Fédérale de Lausanne (CH), University of Turin (IT), Swinburne University of Technology (AU), Case Western Reserve University (US), Technical University of Munich (DE), University of Portsmouth (GB), Lancaster University (GB), Université de Strasbourg (FR), University of Chile (CL), Heidelberg Institute for Theoretical Studies (DE), Ludwig-Maximilians-Universität München (DE), University of Genoa (IT), Sapienza University of Rome (IT), University of the Western Cape (ZA), National Institute for Astrophysics (IT), RWTH Aachen University (DE), Université Grenoble Alpes (FR), University of Bologna (IT), Technical University of Denmark (DK), Aalto University (FI)
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